SUSY DARK MATTER Achille Corsetti and Pran Nath Department Of

View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server SUSY DARK MATTER Achille Corsetti and Pran Nath Department of Physics, Northeastern University, Boston, MA 02115-5005, USA Abstract Several new effects have been investigated in recent analyses of supersymmetric dark matter. These include the effects of the uncertainties of wimp velocity dis- tributions, of the uncertainties of quark densities, of large CP violating phases, of nonuniversalities of the soft SUSY breaking parameters at the unification scale and of coannihilation on supersymmetric dark matter. We review here some of these with emphasis on the effects of nonuniversalities of the gaugino masses at the unification scale on the neutralino-proton cross-section from scalar interactions. The review encompasses several models where gaugino mass nonuniversalities occur including SUGRA models and D brane models. One finds that gaugino mass nonuniversalities can increase the scalar cross-sections by as much as a factor of 10 and also significantly extend the allowed range of the neutralino mass consistent with constraints up to about 500 GeV. These results have important implications for the search for supersymmetric dark matter. 1 INTRODUCTION Over the recent past there has been considerable experimental activity in the direct detection of dark matter 1, 2) and further progress is expected in the ongoing experiments 1, 2, 3) and new experiments that may come online in the future 4). At the same time there have been several theoretical developments which have shed light on the ambiguities and possible corrections that might be associated with the predictions on supersymmetric dark matter. These consist of the effects on the dark matter analyses of wimp velocity 5, 6, 7) and of the rotation of the galaxy 8),the effects of the uncertainties of quark densities 9, 10, 11) and the uncertainties of the SUSY parameters 12), effects of large CP violating phases 13, 14), effects of scalar nonuniversalities 15), effects of nonuniversalities of gaugino masses 11) and effects of coannihilation 16). In this paper we will discuss some of these briefly but mainly focus on the effects of nonuniversalities of the gaugino masses on dark matter. In the Minimal Supersymmetric Standard Model (MSSM) there are 32 supersymmetric particles and with R parity conservation the lowest mass supersymmetric particle (LSP) is absolutely stable. In many unified models, such as in the SUGRA models 17), one finds that the lightest neutralino is the LSP over most of the parameter space of the model. Thus the lightest neutralino is a candidate for cold 2 dark matter. The quantity that constrains supersymmetric models is Ωχh where Ωχ = ρχ/ρc where ρχ is the density of relic neutralinos at the current temperatures, 2 and ρc =3H0 /8πGN is the critical matter density, and h is the Hubble parameter H0 in units of 100 km/sMpc. The most recent measurements of h from the Hubble Space Telescope give 18) h =0.71 0.03 0.07 (1) ± ± 19) Similarly the most recent analyses of Ωm give Ω =0.3 0.08 (2) m ± If we assume that the component of Ω in Ω is Ω 0.05 which appears reasonable, B m B ' then this leads to the result Ω h2 =0.126 0.043. Perhaps a more cautious choice χ ± of the range would be a 2σ range which gives ∼ 0.02 Ω h2 0.3(3) ≤ χ ≤ The quantity of interest theoretically is 3 3 1/2 2 11 Tχ Tγ Nf Ωχh = 2.48 10− (4) ∼ × Tγ 2.73 J(xf ) Here Tf is the freeze-out temperature, xf = kTf /mχ~ where k is the Boltzman constant, N is the number of degrees of freedom at the time of the freeze-out, ( Tχ )3 f Tγ is the reheating factor, and J(xf )isgivenby xf 2 J (xf )= dx συ (x)GeV − (5) Z0 h i where <σv>is the thermal average with σ the neutralino annihilation cross-section and v the neutralino relative velocity. 2 Detection of Milky Way wimps Both direct and indirect methods are desirable and complementary for the detection of Milky Way wimps. We shall focus here on the direct detection. In this case the fundamental detector is the quark and the relevant interactions are the su- pergravity neutralino-quark-squark interactions. The scattering of neutralinos from quarks contains squark poles in the s channel and the Z boson and the Higgs boson (h, H0,A0) poles in the t channel. Since the wimp scattering from quarks is occuring at rather low energies one may, to a good approximation, integrate on the intermediate squark, Z and Higgs poles to obtain a low energy effective Lagrangian which gives a four-Fermi interaction of the following form =¯χγ γ χqγ¯ µ(AP + BP )q + Cχχm¯ qq¯ + Dχγ¯ χm qγ¯ q (6) Leff µ 5 L R q 5 q 5 The contribution of D is generally small and thus the scattering is effectively gov- erned by the terms A,B and C. Analysis of dark matter is affected by several factors. We discuss these briefly below. 2.1 Uncertainties in wimp density and velocity Two of the quantities that control the detection of dark matter are the wimp mass density and the wimp velocity. Estimates of Milky Way wimp density lie in the 20) 3 range ρ =(0.2 0.7)GeV cm− and the event rates in the direct detection χ − depend directly on this density. A second important factor regarding wimps that enters in the dark matter analyses is the wimp velocity. One typically assumes a Maxwellian velocity distribution for the wimps and the current estimates for the rms wimp velocity give v = 270 km/s with, however, a significant uncertainty. Estimates for the uncertainty lie in the range of 24 km/s to 70 km/s 21). A reasonable ± ± estimate then is that the rms wimp velocity lies in the range 21) v = 270 50 km/s (7) ± Analyses including the wimp velocity variations show that the detection rates can have a significant variation, i.e., a factor of 2-3 on either side of the central values 7). 2.2 Effects of uncertainties of quark densities The scattering of neutralinos from quarks are dominated by the scalar interaction which is controlled by the term C in Eq.(6). The dominant part of the scattering thus arises from the scalar part of the χ p cross-section which is given by − 2 4µr p 2 p 2 σχp(scalar)= ( fi Ci + (1 fi ) Ca) (8) π i=Xu,d,s 27 − i=Xu,d,s a=Xc,b,t Here µ is the reduced mass in the χ p system and f p (i=u,d,s quarks) are quark r − i densities inside the proton defined by m f p =<pm q¯ q p> (9) p i | qi i i| p There are significant uncertainties in the determination of fi . To see the range of these uncertainties it is useful to parametrize the quark densities so that 11) p mu σπN fu = (1 + ξ) mu + md mp p md σπN fd = (1 ξ) mu + md − mp p ms σπN fs = (1 x) (10) mu + md − mp wherewehavedefined ¯ ¯ σ0 <puu¯ + dd 2¯ss p> <puu¯ dd p> x = = | −¯ | ,ξ= | − ¯ | σπN <puu¯ + dd p> <puu¯ + dd p> | | 1 | | σ =<p2− (m + m )(¯uu + dd¯ p> (11) πN | u d | 11) The current range of determinations of σπN give σ =48 9 MeV, x =0.74 0.25,ξ=0.132 0.035 (12) πN ± ± ± p With the above range of errors one finds that fi lie in the range f p =0.021 0.004,fp =0.029 0.006,fp =0.21 0.12 (13) u ± d ± s ± p Of these the errors in fs generates the largest variations. A detailed analysis shows that the scalar cross-section can vary by a factor of 5 in either direction due to errors in the quark densities 11). 2.3 CP violation effects on dark matter The soft SUSY breaking parameters that arise in supersymmetric theories after spontaneous breaking are in general complex with phases O(1) and can lead to large electric dipole moment of the electron and of the neutron in conflict with current experiment. Recently a cancellation mechanism was proposed as a possible solution to this problem 22, 23). With the cancellation mechanism the total EDM of the electron and of the neutron can be in conformity with data even with phases O(1) and sparticle masses which are relatively light. The presence of large CP phases can affect dark matter and other low energy phenomena. Effects of CP violating phases on dark matter have been investigated for some time 13) and more recently such analyses have been extended to determine the effects of large CP phases under the cancellation mechanism 14). One finds that the EDM constraints play a crucial role in these analyses. Thus in the absence of CP violating phases one finds that the χ p cross-section can change by orders of magnitude when plotted as a function − of θµ (the phase of µ). These effects are, however, significantly reduced when the constraints arising from the current experimental limits on the electron and on the neutron EDMs are imposed. After the imposition of the constraints the effects of CP violating phases are still quite significant in that the χ p cross-section can vary − by a factor of 2. Thus precision predictions of the χ p cross-section should take ∼ − account of the CP phases if indeed such phases do exist in a given model.

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